Titlebook: General Theory of Light Propagation and Imaging Through the Atmosphere; T. Stewart McKechnie Book 2022Latest edition The Editor(s) (if app

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Michael D. Rucki,Gregory R. Millers the Fourier transform of the product of the atmospheric MTF and the telescope OTF. The seeing disc star images delivered by large (>1 m) telescopes typically measure about 1-arcsec across which, sadly, is about one or two orders of magnitude broader than would be delivered by diffraction-limited v

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https://doi.org/10.1007/978-1-4020-3953-9lence structure functions. To illustrate the crucial importance of turbulence structure size on star image appearance, two wavefront realizations are generated, one where the outer scale is less than one meter, the other where the outer scale is three times larger. Instantaneous images are then calc

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Comparative Studies of Tornado-Like Vorticesuations that describe these images may not be transparent to all readers, in this chapter we simplify the mathematics by approximating star images by best-fitting Gaussian functions. Single Gaussian functions are used to approximate core-only or halo-only images; two summed Gaussian functions are us

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Elementary Theory of Del Pezzo Surfaces,h properties identical to those of actual images obtained by large telescopes in the field. The imaging optic used in the simulator—typically 5 mm in diameter—is designed to provide a suitably scaled replica of the telescope point-spread function. Scaling procedures are also described for designing

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https://doi.org/10.1007/978-94-017-8645-4apon systems. Collimated beams are treated as well as beams that converge to a focus in the atmosphere. For terrestrial laser communication systems, laser beam quality is influenced by atmospheric turbulence and the aberrations of the beam-projection telescope. For HEL beams, other influences includ